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Sommerfeld enhancement and Breit-Wigner enhancement of the dark matterannihilation have been proposed to explain the "boost factor" which issuggested by observed cosmic ray excesses. Although these two scenarios canprovide almost indistinguishable effects on the cosmic ray fluxes, the crosssections of the self-interaction in those enhancement mechanisms aredrastically different. As a result, we show that they can be distinguished byexamining the effects of the self-interaction on the halo shapes. In Sommerfeldenhancement models with m_phi<100MeV and m_DM<3TeV, the self-interaction canleave observable imprints in the galactic dynamics, while dark matter iseffectively collisionless in Breit-Wigner models.

Distinguishing Dark Matter Annihilation Enhancement Scenarios via Halo Shapes